Abstract
The quality of GaiaDR3 proper motions make them suitable for mapping for the first time the 3D velocity field of the Large Magellanic Cloud disc kinematics. These maps show a high degree of complexity and comparison with controlled N-body simulations becomes essential. We plan to use  KRATOS simulations, a suite of 24 LMC-like N-body simulations, to understand the disc kinematics and transform them to a Gaia mock catalogue and/or an Euclid mock catalogue.