  The Andromeda galaxy (M31) contains a box/peanut bulge (BPB) entangled with a
classical bulge (CB) requiring a triaxial modelling to determine the dynamics,
stellar and dark matter mass. We construct made-to-measure models fitting new
VIRUS-W IFU bulge stellar kinematic observations, the IRAC-3.6$\mu$m
photometry, and the disc's HI rotation curve. We explore the parameter space
for the 3.6$\mu$m mass-to-light ratio $(\Upsilon_{3.6})$, the bar pattern speed
($\Omega_p$), and the dark matter mass in the composite bulge ($M^B_{DM}$)
within 3.2kpc. Considering Einasto dark matter profiles, we find the best
models for $\Upsilon_{3.6}=0.72\pm0.02\,M_\odot/L_\odot$,
$M^B_{DM}=1.2^{+0.2}_{-0.4}\times10^{10}M_\odot$ and
$\Omega_p=40\pm5\,km/s/kpc$. These models have a dynamical bulge mass of
$M_{dyn}^B=4.25^{+0.10}_{-0.29}\times10^{10}M_{\odot}$ including a stellar mass
of $M^B=3.09^{+0.10}_{-0.12}\times10^{10}M_\odot$(73%), of which the CB has
$M^{CB}=1.18^{+0.06}_{-0.07}\times10^{10}M_\odot$(28%) and the BPB
$M^{BPB}=1.91\pm0.06\times10^{10}M_\odot$(45%). We also explore models with NFW
haloes finding that, while the Einasto models better fit the stellar
kinematics, the obtained parameters agree within the errors. The $M^B_{DM}$
values agree with adiabatically contracted cosmological NFW haloes with M31's
virial mass and radius. The best model has two bulge components with completely
different kinematics that only together successfully reproduce the observations
($\mu_{3.6},\upsilon_{los},\sigma_{los},h3,h4$). The modelling includes dust
absorption which reproduces the observed kinematic asymmetries. Our results
provide new constraints for the early formation of M31 given the lower mass
found for the classical bulge and the shallow dark matter profile, as well as
the secular evolution of M31 implied by the bar and its resonant interactions
with the classical bulge, stellar halo and disc.
