  Context. Asteroseismic studies showed that cores of post main-sequence stars
rotate slower than theoretically predicted by stellar models with purely
hydrodynamical transport processes. Recent studies on main sequence stars,
particularly Gamma Doradus ($\gamma$ Dor) stars, revealed their internal
rotation rate for hundreds of stars, offering a counterpart on the main
sequence for studies of angular momentum transport. Aims. We investigate
whether such a disagreement between observed and predicted internal rotation
rates is present in main sequence stars by studying angular momentum transport
in $\gamma$ Dor stars. Furthermore, we test whether models of rotating stars
with internal magnetic fields can reproduce their rotational properties.
Methods. We compute rotating models with the Geneva stellar evolution code
taking into account meridional circulation and the shear instability. We also
compute models with internal magnetic fields using a general formalism for
transport by the Tayler-Spruit dynamo. We then compare these models to
observational constraints for $\gamma$ Dor stars that we compiled from the
literature, combining so the core rotation rates, projected rotational
velocities from spectroscopy, and constraints on their fundamental parameters.
Results. We show that combining the different observational constraints
available for $\gamma$ Dor stars enable to clearly distinguish the different
scenarios for internal angular momentum transport. Stellar models with purely
hydrodynamical processes are in disagreement with the data whereas models with
internal magnetic fields can reproduce both core and surface constraints
simultaneously. Conclusions. Similarly to results obtained for subgiant and red
giant stars, angular momentum transport in radiative regions of $\gamma$ Dor
stars is highly efficient, in good agreement with predictions of models with
internal magnetic fields.
