  In order to explore how the early internal rotational properties of star
clusters are affected by the external potential of their host galaxies, we have
run a suite of $N$-body simulations following the early dynamical evolution and
violent relaxation of rotating star clusters embedded in a tidal field. Our
study focuses on models for which the cluster's rotation axis has a generic
orientation relative to the torque of the tidal field. The interaction between
the violent relaxation process, angular momentum of the cluster, and the
external torque creates a complex kinematic structure within the cluster, most
prominently a radial variation in the position of the rotation axis along both
the polar and azimuthal directions. We also examine the cluster's velocity
dispersion anisotropy and show that the projected anisotropy may be affected by
the variation of the rotation axis directions within the cluster; the
combination of projection effects and the complex kinematical features may
result in the measurement of tangential anisotropy in the cluster's inner
regions. We also characterize the structural properties of our clusters as a
function of their initial rotation and virial ratio and find that clusters may
develop a triaxial morphology and a radial variation of the minor axis not
necessarily aligned with the rotation axis. Finally, we examine the long-term
evolution of these complex kinematic features.
