The |$\rm {H}\alpha$| -to-UV luminosity ratio (|$L(\text{H}\alpha)/L(\rm UV)$|) is often used to probe bursty star formation histories (SFHs) of star-forming galaxies and it is important to validate it against other proxies for burstiness. To address this issue, we present a statistical analysis of the resolved distribution of star formation rate surface density (ΣSFR) as well as stellar age and their correlations with the globally measured |$L(\text{H}\alpha)/L(\rm UV)$| for a sample of 310 star-forming galaxies in two redshift bins of 1.37 < z < 1.70 and 2.09 < z < 2.61 observed by the MOSFIRE Deep Evolution Field (MOSDEF) survey. We use the multiwaveband CANDELS/3D-HST imaging of MOSDEF galaxies to construct ΣSFR and stellar age maps. We analyse the composite rest-frame far-ultraviolet spectra of a subsample of MOSFIRE Deep Evolution Field (MOSDEF) targets obtained by the Keck Low Resolution Imager and Spectrometer (LRIS), which includes 124 star-forming galaxies (MOSDEF-LRIS) at redshifts 1.4 < z < 2.6, to examine the average stellar population properties, and the strength of age-sensitive far-ultraviolet spectral features in bins of |$L(\text{H}\alpha)/L(\rm UV)$|. Our results show no significant evidence that individual galaxies with higher |$L(\text{H}\alpha)/L(\rm UV)$| are undergoing a burst of star formation based on the resolved distribution of ΣSFR of individual star-forming galaxies. We segregate the sample into subsets with low and high |$L(\text{H}\alpha)/L(\rm UV)$|. The high- |$L(\text{H}\alpha)/L(\rm UV)$| subset exhibits, on average, an age of |$\log [\rm {Age/yr}]$| = 8.0, compared to |$\log [\rm {Age/yr}]$| = 8.4 for the low- |$L(\text{H}\alpha)/L(\rm UV)$| galaxies, though the difference in age is significant at only the 2σ level. Furthermore, we find no variation in the strengths of Si iv λλ1393, 1402 and C iv λλ1548, 1550 P-Cygni features from massive stars between the two subsamples, suggesting that the high- |$L(\text{H}\alpha)/L(\rm UV)$| galaxies are not preferentially undergoing a burst compared to galaxies with lower |$L(\text{H}\alpha)/L(\rm UV)$|. On the other hand, we find that the high- |$L(\text{H}\alpha)/L(\rm UV)$| galaxies exhibit, on average, more intense He ii λ1640 emission, which may possibly suggest the presence of a higher abundance of high-mass X-ray binaries. [ABSTRACT FROM AUTHOR]