In NGC 4244, we find a flattened nuclear star cluster with multiple components, a younger disk structure and an older spheroidal structure (Paper I). From our NIFS data, we have shown that the cluster is rotating at $\pm$30 kms$^{-1}$ within the central 10 pc of the cluster. This rotation is not confined just to the younger disk component, but also appears to be present in the older, more spheroidal component.

There are two basic models for NSC formation: (1) globular clusters which collect at the center due to dynamical friction [@tremaine75; @lotz01], or (2) episodic accretion of gas onto the center followed by [*in situ*]{} star formation [@milosavljevic04; @bekki07]. A third alternative (3), combining these two scenarios, has recently been proposed by Milosavljevic & Agarwal (2008, [*private communication*]{}) in which NSCs form from young star clusters in the inner part of the galaxy disk which are massive enough to accrete onto the nucleus. These mechanisms are not exclusive; NSCs could form from a combination of these effects, and different types of galaxies may have different dominant mechanisms. However, our observations for NGC 4244 strongly conflict with the first scenario. If a significant fraction of the NSC were formed from globular 