  The radial velocities of the 13 globular clusters in the Large Magellanic
Cloud have a dispersion of 28 km s$^{-1}$ relative to the HI rotation curve of
the LMC, compared to a dispersion of 30 km s$^{-1}$ with regard to the mean
globular cluster velocity. This shows that, contrary to a suggestion by
Schommer et al. (1992), one cannot yet rule out the possibility that the LMC
globular clusters formed in a pressure supported halo, rather than in rotating
disk. The globular clusters in the LMC may therefore, after all, exhibit a
relationship between age and kinematics that is similar to that of the clusters
in M33.
