Cosmological hydrodynamical simulations are rich tools to understand the role and impact of galaxy environment and mergers, and gas dynamics and stellar kinematics in galaxy formation and evolution. However, these simulations require some level of calibration to observations. In this talk, I will compare predictions at z=0 from the Eagle, Hydrangea, Horizon-AGN, and Magneticum simulations with IFS data from the SAMI Galaxy Survey, ATLAS-3D, CALIFA and MASSIVE surveys. The main goal of our work is to simultaneously compare structural, dynamical, and stellar population measurements, in order to identify key areas of success and tension. I will show that our comparison between simulations and observational data has highlighted several areas for improvement, such as the need for improved modelling resulting in a better vertical disk structure. Yet these results that I will present, will demonstrate the vast improvement of cosmological simulations in recent years.