  We report statistical results for dark matter (DM) velocity anisotropy,
\beta, from a sample of some 6000 cluster-size halos (at redshift zero)
identified in a \Lambda CDM hydrodynamical adaptive mesh refinement simulation
performed with the Enzo code. These include profiles of \beta\ in clusters with
different masses, relaxation states, and at several redshifts, modeled both as
spherical and triaxial DM configurations. Specifically, although we find a
large scatter in the DM velocity anisotropy profiles of different halos (across
elliptical shells extending to at least ~$1.5 r_{vir}$), universal patterns are
found when these are averaged over halo mass, redshift, and relaxation stage.
These are characterized by a very small velocity anisotropy at the halo center,
increasing outward to about 0.27 and leveling off at about $0.2 r_{vir}$.
Indirect measurements of the DM velocity anisotropy fall on the upper end of
the theoretically expected range. Though measured indirectly, the estimations
are derived by using two different surrogate measurements - X-ray and galaxy
dynamics. Current estimates of the DM velocity anisotropy are based on very
small cluster sample. Increasing this sample will allow testing theoretical
predictions, including the speculation that the decay of DM particles results
in a large velocity boost. We also find, in accord with previous works, that
halos are triaxial and likely to be more prolate when unrelaxed, whereas
relaxed halos are more likely to be oblate. Our analysis does not indicate that
there is significant correlation (found in some previous studies) between the
radial density slope, \gamma, and \beta\ at large radii, $0.3 r_{vir} < r <
r_{vir}$.
