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Previous full-lifetime simulations of single-star multi-planet systems acrossall phases of stellar evolution have predominately assumed coplanar ornearly-coplanar orbits. Here we assess the consequences of this assumption byremoving it and exploring the effect of giant branch mass loss on the stabilityof two-planet systems with small to moderate non-Kozai (<40 degrees) relativeinclinations. We run nearly 10^4 simulations over 14 Gyr for F-star, A-star andB-star planet hosts, incorporating main sequence stellar masses of 1.5, 2.0,2.5, 3.0 and 5.0 solar masses, and initial planetary semimajor axis ratios thatstraddle their three-dimensional Hill stability limits. We find that thenear-coplanar assumption can approximate well the stability frequencies andcritical separations found for higher inclinations, except around strongmean-motion commensurabilities. Late instabilities -- after the star has becomea white dwarf -- occur throughout the explored mutual inclination range.Consequently, non-Kozai mutual inclination should not be used as a predictiveorbital proxy for determining which white dwarf multi-planet systems discoveredby Gaia should represent high-priority follow-up targets for the detection ofmetal pollution and planetary debris discs.

Effects of non-Kozai mutual inclinations on two-planet system stability through all phases of stellar evolution