Gamma Doradus stars are A-F type main sequence stars which pulsate in high-order non-radial gravity modes. These modes uniquely probe the deep stellar interior and reveal the properties of the near-core region. The period spacing patterns of g-mode pulsations have been successfully used as observable indicators to constrain the surface-to-core rotation for individual stars. Pulsation frequencies of gamma Doradus stars are comparable to their rotation frequencies and hence their oscillations are strongly coupled with the effects induced by rotation. Various theoretical formalisms have been introduced to describe interior rotation by applying approximations to the physics of stellar oscillations, in particular, the treatment of the Coriolis force and centrifugal effects. We investigate the ability of g-modes to differentiate between two different rotation formalisms using a grid of 1D stellar models computed with the MESA evolution code. The code simulates the adiabatic oscillations of gamma Doradus stars and provides the period spacings for each model. With detailed analysis on the grids we can evaluate the extent to which the two rotation formalisms are distinguishable in observational data. This will allow us to improve seismic modelling for rotating gamma Doradus stars and extend our capabilities to trace the interior stellar structure.