The observed dynamical parameters of the Magellanic Clouds (MCs) clusters are derived by means of star counts. There are many rich globular, young disk clusters in the MCs with no counterparts in our galaxy. The old clusters were found statistically less extended with systematically smaller total masses than those of the galactic globulars. So it is worth emphasizing that clusters of all ages (from stellar evolution point of view) are detected in the MCs with very large total number of stars and structural parameters characterising the old halo galactic globulars.
The radial density profiles of these stellar systems were used for deriving information on their dynamical stage. Some of the clusters indicate mass segregation of post core collapse profiles, giving evidence for a two body relaxation mechanism. Nevertheless some very young clusters show well relaxed profiles with evolutionary ages too short for a two body relaxation mechanism, so that the
shape of their profiles is due to their initial relaxation.
A number of clusters were found with an unexpected distortion in the outer areas of their density profiles at systematically constant distances to their centres. It is probable that an halo is formed around these clusters giving evidence that the morphology of the MCs may favorite the occurence of such effects.
The dynamical evolution of star clusters is discussed. We investigate especially the possible disruption of globular clusters by massive black holes, which have been proposed as the major constituents of dark galactic coronae. As an example, we discuss here the globular clusters in the elliptical galaxy M87. The proposed massive black holes could be responsible for the observationally indicated depletion of the globular cluster system in the inner parts of M87 with respect to the stellar light distribution of this galaxy.