  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) =
(102.40 +/- 1.02 & -4.60 +/- 0.47; NGC 5999), (96.69 +/- 1.10 & -0.58 +/-
0.045; UFMG 1), (97.47 +/- 1.09 & 1.56 +/- 0.051; UFMG 2), and (98.65 +/- 1.12
& -0.26 +/- 0.060; UFMG 3). On the other hand, Velocity Ellipsoid Parameters
VEPs for those are also computed; e.g. space velocities due to Galactic
coordinates, dispersion velocities (sigma_1, sigma_2, sigma_3) due to matrix
elements for all ij, projected distances (X_sun, Y_sun, Z_sun) on the plane
disc, and the Solar elements (S_sun, 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 MC; including total
number of main-sequence NMS and non-main-sequence Nnon-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. tau >> 1), and the fourth one
in non-relaxed.
