  We investigate the evolution of a multi--planet--disc system orbiting one
component of a binary star system. The planet--disc system is initially
coplanar but misaligned to the binary orbital plane. The planets are assumed to
be giants that open gaps in the disc. We first study the role of the disc in
shaping the mutual evolution of the two planets using a secular model for low
initial tilt. In general we find that the planets and the disc do not remain
coplanar, in agreement with Lubow & Martin (2016) for the single planet case.
Instead, the planets and the disc undergo tilt oscillations. A high mass disc
between the two planets causes the planets and the disc to nodally precess at
the same average rate but they are generally misaligned. The amplitude of the
tilt oscillations between the planets is larger while the disc is present. We
then consider higher initial tilts using hydrodynamical simulations and explore
the possibility of the formation of eccentric Kozai-Lidov (KL) planets. We find
that the inner planet's orbit undergoes eccentricity growth for a large range
of disc masses and initial misalignments. For a low disc mass and large initial
misalignment both planets and the disc can undergo KL oscillations.
Furthermore, we find that sufficiently massive discs can cause the inner planet
to increase its inclination beyond $90^{\circ}$ and therefore to orbit the
binary in a retrograde fashion. The results have important implications for the
explanation of very eccentric planets and retrograde planets observed in
multi-planet systems.
