Magnetospheric accretion of circumstellar disc material is a mechanism that affects a variety of astrophysical objects, from young low-mass stellar objects to compact objects, such as white dwarves and neutron stars. Within this picture, the accretion flow in their inner circumstellar disc is channeled along the stellar magnetic field lines and ultimately shocks the stellar surface, inducing an exchange of mass, angular momentum and energy that can spin up/down the star itself and modify its intrinsic evolution. We will look at preliminary results of non-ideal 2.5-dimensional simulations of the surroundings of magnetised rotating young stars and explore how different parameters of the problem can affect the accretion dynamics and change their spin evolution and emission properties.