  HD 113337 and HD 38529 host pairs of giant planets, a debris disc, and wide
M-type stellar companions. We measure the disc orientation with resolved images
from Herschel and constrain the three-dimensional orbits of the outer planets
with Gaia DR2 and Hipparcos astrometry. Resolved disc modelling leaves
degeneracy in the disc orientation, so we derive four separate planet-disc
mutual inclination ($\Delta I$) solutions. The most aligned solutions give
$\Delta I=17-32\deg$ for HD 113337 and $\Delta I=21-45\deg$ for HD 38529 (both
1$\sigma$). In both systems, there is a small probability (<0.3 per cent) that
the planet and disc are nearly aligned ($\Delta I < 3\deg$). The stellar and
planetary companions cause the orbits of disc material to precess about a plane
defined by the forced inclination. We determine this as well as the precession
time-scale to interpret the mutual inclination results. We find that the debris
discs in both systems could be warped via joint influences of the outer planet
and stellar companion, potentially explaining the observed misalignments.
However, this requires HD 113337 to be old (0.8-1.7 Gyr), whereas if young
(14-21 Myr), the observed misalignment in HD 113337 could be inherited from the
protoplanetary disc phase. For both systems, the inclination of the stellar
spin axis is consistent with the disc and outer planet inclinations, which
instead supports system-wide alignment or near alignment. High-resolution
observations of the discs and improved constraints on the planetary orbits
would provide firmer conclusions about the (mis)alignment status.
