Impact cratering is an important process in the formation and evolution of the Solar System. Planetary crusts have been shaped by intense impact bombardment from the first few hundred million to more than a billion years after planet formation. It is a reasonably well understood physical phenomena, resulting in the formation of impact craters with varying morphology depending on the properties of the impact (e.g., impact speed and projectile size) and target (e.g., crustal composition and thermal regime at the impact site). Therefore, it can reveal valuable information regarding the crustal properties and internal structure during the impact bombardment period. Through comparison of impact modelling simulations with available space exploration data, remote observations, and geophysical modelling, it is possible to establish constrains on the crustal properties of the parent body, making them a valuable scientific tool for understanding the geological evolution of objects with solid surfaces. On Mars, these simulations can be used to improve the current understanding of the planet’s crustal properties at the time of impact basin formation through the definition of scaling relations and comparisons with geological data available in the literature, including the latest results from NASA’s InSight mission. This work aims to present a brief overview of this methodology, including preliminary results of an ongoing investigation of Mars’ impact basins.