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We present a detailed dynamical analysis of the projected density andkinematical data available for the globular cluster Omega Cen. We solve thespherical anisotropic Jeans equation to predict the projected profiles of theRMS velocity in each of the three orthogonal coordinate directions (line ofsight, proper motion radial, and proper motion tangential). We fit the modelsto new HST star count and proper motion data near the cluster center presentedin Paper I, combined with existing ground-based measurements. We also deriveand model the Gauss-Hermite moments of the observed proper motiondistributions. The projected density profile is consistent with being flat nearthe center, with an upper limit gamma=0.07 on the central logarithmic slope.The RMS proper motion profile is also consistent with being flat near thecenter, and there are no unusually fast-moving stars. The models provide a goodfit and yield a 1-sigma upper limit MBH < 1.2E4 solar masses on the mass of apossible intermediate-mass black hole (IMBH). The inferred upper limitcorresponds to MBH/Mtot < 0.43%. We combine this with results for otherclusters and discuss the implications for globular cluster IMBH demographics.Tighter limits will be needed to rule out or establish whether globularclusters follow the same black hole demographics correlations as galaxies. Thearguments put forward by Noyola et al. (2008) to suspect an IMBH in Omega Cenare not confirmed by our study; the IMBH mass they suggested is firmly ruledout.

New Limits on an Intermediate Mass Black Hole in Omega Centauri: II. Dynamical Models