The work on the kinematical parameters and spatial shape structure have been performed with Gaia DR2 astrometry data of the new recently southern discovered open clusters; UFMG 1, UFMG 2, and UFMG 3 in the vicinity ( 1.3 degrees radius) of the rarely studied NGC 5999. The apexes positions with AD-diagram method are computed for about 107, 168, 98, and 154 members of these star clusters, respectively, our calculated values of apex coordinates, seems like: (A, D) = (102 o .40 ± 1.02 & -4 o .60 ± 0.47; NGC 5999), (96 o .69 ± 1.10 & -0 o .58 ± 0.045; UFMG 1), (97 o .47 ± 1.09 & 1 o .56 ± 0.051; UFMG 2), and (98 o .65 ± 1.12 & -0 o .26 ± 0.060; UFMG 3). On the other hand, Velocity Ellipsoid Parameters VEPs for those are also computed; e.g. space velocities U, V, W due to Galactic coordinates, dispersion velocities ( 1 , 2 , 3 )due to matrix elements ij , projected distances (X , Y , Z ) on the plane disc, and the Solar elements (S , l A , b A ). According to an approximation of spatial and kinematical shape, UFMGs and NGC 5999 seem to have a spatial difference in their space locations but they appear to have formed in the same region of the Galactic disc. The total cumulative mass M C ; including total number of main-sequence N MS and nonmain-sequence N non-MS of these clusters also evaluated here with a second-order polynomial of mass-luminosity relation in order to get clusters tidal radii (pc). Finally, we concluded that NGC 5999, UFMG 1, and UFMG 2 are dynamically relaxed (i.e. >> 1), and the fourth one in non-relaxed.