In this talk, I will present results of our recent 3D GRHD simulations of thick accretion disks around tilted Kerr black holes. We investigate the effects of the tilt angle between the disk angular momentum vector and black hole spin on the dynamics of these systems, being particularly interested in a possible imprint of the tilt angle in the gravitational wave pattern as the torus evolves in the tilted spacetime. We find that Papalouizou-Pringle unstable models still develop the PPI when the central BH is tilted. For the models where the PPI saturates abruptly, the central BH is given a mild kick. We simulate the systems using the Einstein Toolkit, using the thorn McLachlan for the evolution of the spacetime via the BSSN formalism and the thorn GRHydro for the evolution of the hydrodynamics, using a 3D Cartesian mesh with adaptive mesh refinement (AMR).