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We have determined bulk proper motions (PMs) for 31 LMC GCs from Gaia eDR3and Hubble Space Telescope data using multiple independent analysis techniques.Combined with literature values for distances, line-of-sight velocities andexisting bulk PMs, we extract full 6D phase-space information for 32 clusters,allowing us to examine the kinematics of the LMC GC system in detail. Exceptfor two GCs (NGC 2159 and NGC 2210) for which high velocities suggest they arenot long-term members of the LMC system, the data are consistent with aflattened configuration that rotates like the stellar disk. The one-dimensionalvelocity dispersions are of order 30 km/s, similar to that of old stellarpopulations in the LMC disk. Similar to the case for Milky Way disk clusters,the velocity anisotropy is such that the dispersion is smallest in theazimuthal direction; however, alternative anisotropies cannot be ruled out dueto distance uncertainties. The data are consistent with a singlemulti-dimensional Gaussian velocity distribution. Given the non-collisionalnature of the LMC disk, this suggests that most, if not all, of the LMC GCs areformed by a single formation mechanism in the stellar disk, despite asignificant spread in age and metallicity. Any accreted halo GC population isabsent or far smaller in the LMC compared to the Milky Way.

Kinematic Structure of the Large Magellanic Cloud Globular Cluster System from Gaia eDR3 and Hubble Space Telescope Proper Motions