This study is concerned with the relative helium abundance variations, as well as other solar wind plasma and interplanetary magnetic field parameters, inside interplanetary coronal mass ejections on medium spatial scales (105–106 km). The analysis is based on long-term WIND spacecraft measurements. It is shown that those scales lack an unambiguous anticorrelation between the helium abundance and plasma parameter β that was revealed on spatial scales greater than 106 km. Events with significant positive and negative correlations are observed with the same probability. In this case, both types of structures can be observed: structures in which the helium abundance grows simultaneously with an increase in the interplanetary magnetic field that are similar to those observed on large scales, as well as structures in which the helium abundance increases with a decline in the interplanetary magnetic field. [ABSTRACT FROM AUTHOR]