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We employ Gaia DR2 proper motions for 151 Milky Way globular clusters fromVasiliev (2019) in tandem with distances and line-of-sight velocities to derivetheir kinematical properties. To assign clusters to the Milky Way thick disk,bulge, and halo we follow the approach of Posti et al. (2018) who distinguishedamong different Galactic stellar components using stars's orbits. Inparticular, we use the ratio $L_{z}/e$, the $Z$ projection of the angularmomentum to the eccentricity, as population tracer, which we complement withchemical abundances extracted from the literature and Monte-Carlo simulations.We find that 20 globular clusters belong to the bar/bulge of the Milky Way, 35exhibit disk properties, and 96 are members of the halo. Moreover, we find thathalo globular clusters have close to zero rotational velocity with averagevalue $<\Theta>$ =1$\pm$ 4 km s$^{-1}$. On the other hand, the sample ofclusters that belong to the thick disk possesses a significant rotation withaverage rotational velocity 179 $\pm$ 6 km s$^{-1}$. The twenty globularclusters orbiting within the bar/bulge region of the Milky Way galaxy haveaverage rotational velocity of 49 $\pm$ 11 km s$^{-1}$.

Milky Way Subsystems from Globular Clusters Kinematics Using Gaia DR2 and HST Data