  Recent studies have shown that AGN discs can host sources of gravitational
waves. Compact binaries can form and merge in AGN discs through their
interactions with the gas and other compact objects in the disc. It is also
possible for the binaries to shorten the merging timescale due to eccentricity
excitation caused by perturbations from the supermassive blackhole (SMBH). In
this paper we focus on effects due to precession-induced (eviction-like)
resonances, where nodal and apsidal precession rates of the binary is
commensurable with the mean motion of the binary around the SMBH. We focus on
intermediate mass black hole (IMBH)-stellar mass black hole (SBH) binaries, and
consider binary orbit inclined from the circum-IMBH disk which leads to the
orbital $J_2$ precession. We show that if a binary is captured in these
resonances and is migrating towards the companion, it can undergo large
eccentricity and inclination variations. We derive analytical expressions for
the location of fixed points, libration timescale and width for these
resonances, and identified two resonances in the near coplanar regime (the
evection and eviction resonances) as well as two resonances in the near polar
regime that can lead to mergers. We also derive analytical expressions for the
maximum eccentricity that a migrating binary can achieve for given initial
conditions. Specifically, the maximum eccentricity can reach 0.9 when captured
in these resonances before orbital decay due to gravitational wave emission
dominates, and the capture is only possible for slow migration ($\sim 10$ Myr)
2-3 order of magnitude longer than the resonance libration timescale. We also
show that capture into multiple resonances is possible, and can further excite
eccentricities.
