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We present the dynamical evolution of ten open clusters which were part ofour previous studies. These clusters include both young and intermediate-ageopen clusters with ages ranging from 25$\pm$19 Myr to 1.78$\pm$0.20 Gyr. Thetotal mass of these clusters ranges from 356.18$\pm$142.90 to1811.75$\pm$901.03 M$_{\odot}$. The Galactocentric distances to the clustersare in the range of 8.91$\pm$0.02 to 11.74$\pm$0.18 kpc. The study is based onthe ground-based UBVRI data supplemented by the astrometric data from the Gaiaarchive. We studied the minimum spanning tree of the member stars for theseclusters. The mass segregation in these clusters was quantified by masssegregation ratios calculated from the mean edge length obtained through theminimum spanning tree. The clusters NGC 2360, NGC 1960, IC 1442, King 21, andSAI 35 have ${\Gamma}_{MSR}$ to be 1.65$\pm$0.18, 1.94$\pm$0.22, 2.21$\pm$0.20,1.84$\pm$0.23, and 1.96$\pm$0.25, respectively which indicate moderate masssegregation in these clusters. The remaining five clusters are found to exhibitweak or no mass segregation. We used the ratio of half mass radius to the tidalradius i.e. R$_{h}$/R$_{t}$ to investigate the effect of the tidal interactionson the cluster structure and dynamics. The ratios of half mass radii to tidalradii are found to be positively correlated with the Galactocentric distanceswith a linear slope of 0.06$\pm$0.01 having linear regression coefficientr-square = 0.93 for the clusters.

The statistical analysis of the dynamical evolution of the open clusters