In part due to the Gaia Revolution, we have made major progress towards a complete phase space portrait of star clusters, and revealed that bulk rotation of the cluster is an integral part of its dynamical history and evolution. The dynamical origin of rotation and why in some observed clusters there is a radial variation of the direction of the rotation axis are still a matter of investigation. This poster presents some of the results of N-body simulations investigating how the early internal rotational properties of star clusters are affected by the external potential of their host galaxies. We also show a possible kinematic signature of dynamically young star clusters.