It is believed that stellar systems become mass-segregated on a time scale comparable to the two-body relaxation time (Tr). Globular clusters in the Magellanic Clouds have an extensive range in age and richness. Thus, in the clouds, there are candidate clusters with ratios of Tr to age both > 1 and < 1. Our objective is to study the radial density structure of clusters as a function of mass (magnitude) and compare with expectations based upon Tr. We report here preliminary results on two such clusters at the age extremes in our sample: NGC 458 (SMC) and 121SCO3 (LMC).