  V892 Tau is a young binary star surrounded by a circumbinary disc which show
hints of interaction with the low-mass nearby star V892 Tau NE. The goal of
this paper is to constrain the orbit of V892 Tau NE and to determine the
resulting circumbinary disc dynamics. We present new ALMA observations of the
V892 Tau circumbinary disc at a twice higher angular and spectral resolution.
We model the data with V892 Tau as a triple system and perform a grid of
hydrodynamical simulations testing several orbits of the companion. The
simulation outputs are then post-processed to build synthetic maps that we
compare to the observations. The 12CO emission of the disc shows clear
non-Keplerian features such as spiral arms. When comparing the data with our
synthetic observations, we interpret these features as ongoing interactions
with the companion. Our simulations indicate that an eccentricity of 0.5 of the
companion is needed to reproduce the observed disc extent and that a mutual
inclination of approximately 60{\deg} with the inner binary reproduces the
measured disc tilt. In order to explain most of the features of the
circumbinary disc, we propose that V892 Tau NE follows a misaligned eccentric
orbit, with an eccentricity between 0.2 and 0.5 and a mutual inclination
between 30{\deg} and 60{\deg}. Such a misaligned companion suggests the disc is
oscillating and precessing with time, stabilising in an intermediate plane with
a non-zero mutual inclination with the inner binary. Given that orbital
configuration, we show that the stability of future planets is compromised in
the second half of the disc once the gas has dissipated.
