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In this paper, we continue our study of the motion of spinning test bodiesorbiting Kerr black holes. Non-spinning test bodies follow geodesics of thespacetime in which they move. A test body's spin couples to the curvature ofthat spacetime, introducing a "spin-curvature force" which pushes the body'sworldline away from a geodesic trajectory. The spin-curvature force is animportant example of a post-geodesic effect which must be modeled carefully inorder to accurately characterize the motion of bodies orbiting black holes. Onemotivation for this work is to understand how to include such effects in modelsof gravitational waves produced from the inspiral of stellar mass bodies intomassive black holes. In this paper's predecessor, we describe a technique forcomputing bound orbits of spinning bodies around black holes with afrequency-domain description which can be solved very precisely. In that paper,we present an overview of our methods, as well as present results for orbitswhich are eccentric and nearly equatorial (i.e., the orbit's motion is no morethan $\mathcal{O}(S)$ out of the equatorial plane). In this paper, we applythis formulation to the fully generic case -- orbits which are inclined andeccentric, with the small body's spin arbitrarily oriented. We compute thetrajectories which such orbits follow, and compute how the small body's spinaffects important quantities such as the observable orbital frequencies$\Omega_r$, $\Omega_\theta$ and $\Omega_\phi$.

Precisely computing bound orbits of spinning bodies around black holes II: Generic orbits