  We use optical spectroscopy from VLT/MUSE, as well as photometric
observations from HST and VLT/HAWK-I, to study the morpho-kinematics of 17 low
mass MACS J0416.1-2403 cluster galaxies at R200 and 5 field galaxies with a
redshift of z~0.4. By measuring fluxes of emission lines, we have recovered the
star formation rates, gas-phase metallicities and the spatially resolved gas
kinematics. We have analysed the structure and morphology of the galaxies from
the photometric data, performing a multi-component decomposition into a bulge
and a disk. The spatially resolved gas velocity fields were modelled using a 3D
approach, which allowed us to retrieve their intrinsic gas kinematics,
including the maximum rotation velocity and velocity dispersion. The cluster
and field population can be classified as star forming main-sequence galaxies,
with only a sub-sample of 4 quenched systems. The lowest mass systems deviate
from the predictions of the fundamental metallicity relation, showing higher
metallicities, whereas the higher mass ones are in accordance with the model
predictions. This might hint at the cut-off of pristine gas inflow and/or the
removal of the hot halo gas as the mechanisms driving these offsets. Our
morpho-kinematic analysis reveals a sub-sample of dwarfs with maximum
velocities vmax <50 km/s, which depart from the Tully-Fisher relation. This
might indicate that their interstellar medium is affected by ram pressure
stripping. However, ~30% of the cluster galaxies have rotation-dominated gas
disks and follow the Tully-Fisher relation. In the stellar mass-S0.5 plane, the
systems follow a tight sequence, with only a sub-population of 5 galaxies
strongly departing from this relation. Both the morphology and kinematics of
the outlier galaxies hint at a combination of pre-processing and
cluster-specific interactions affecting their stellar and gas disks.
