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 very young LMC clusters SL666, NGC2098 and NGC2100 were found to exhibit a variation of spectral types with distance from the cluster centre. From spectral dassification of their bright members it is found that the early type stars are accumulated in the inner region of the cluster whereas the late type ones are found in the outer areas. Star counts on photographic plates with different exposure times have shown that the bright stars are segregated in the central regions of the clusters. Both observational results from spectral classlfication and star counts give evidence that the most massive early type stars are located in the inner parts of the clusters. This allow us to suggest that the observed mass segregation is not due
to the relaxation mechanism of the clusters.