The lensing effect, i.e. the bending of light by matter along the line of sight from the source to the observer, depends only on the mass distribution of the intervening structures, making gravitational lensing an ideal tool for measuring the mass profiles of lensing structures, from galaxy to cosmological scales. Of particular interest for cosmology is the detailed distribution of mass in galaxy clusters and groups, which provides important clues to their formation and assembly, as well as a test of the cosmological models. In this talk, i will show how different and complementary regimes of gravitational lensing can be used to map the dark matter distribution in galaxy clusters and groups on different scales (from the sub-halo scale to the whole structure). I will present some results obtained on different structures and will compare to the expectations from dedicated N-body numerical simulations. Aware of both the complexity of these structure and the limitations of gravitational lensing, I will discuss the relevance of a multi-probe approach that combines different measurements of the gravitational potential we aim to investigate.