  The physics of stellar rotation plays a crucial role in the evolution of
stars, their final fate and the properties of compact remnants. Diverse
approaches have been adopted to incorporate the effects of rotation in stellar
evolution models. This study seeks to explore the consequences of these various
prescriptions for rotation on essential outputs of massive star models. We
compute a grid of 15 and 60 M$_{\odot}$ stellar evolution models with the
Geneva Stellar Evolution Code (GENEC), accounting for both hydrodynamical and
magnetic instabilities induced by rotation. In both the 15 and 60 M$_{\odot}$
models, the choice of the vertical and horizontal diffusion coefficients for
the non magnetic models strongly impacts the evolution of the chemical
structure, but has a weak impact on the angular momentum transport and the
rotational velocity of the core. In the 15 M$_{\odot}$ models, the choice of
diffusion coefficient impacts the convective core size during the core
H-burning phase, whether the model begins core He-burning as a blue or red
supergiant and the core mass at the end of He-burning. In the 60 M$_{\odot}$
models, the evolution is dominated by mass loss and is less affected by the
choice of diffusion coefficient. In the magnetic models, magnetic instability
dominates the angular momentum transport and such models are found to be less
mixed when compared to their rotating non-magnetic counterparts. Stellar models
with the same initial mass, chemical composition, and rotation may exhibit
diverse characteristics depending on the physics applied. By conducting
thorough comparisons with observational features, we can ascertain which
method(s) produce the most accurate results in different cases.
