Magnetic reconnection releases energy explosively as fields are reconfigured in plasmas ranging from solar flares to planetary magnetospheres and a growing number of astrophysical applications. While considerable progress has been made within 2D models, very little is known regarding the influence of realistic 3D dynamics. The recent advent of petascale computing has greatly expanded the range of feasible kinetic simulations that permit a first-principles description. These simulations are leading to some major breakthroughs in our understanding of magnetic reconnection and the generation of turbulence. This talk will highlight some key results from this recent work with an emphasis on parameter regimes relevant to the Earth’s magnetosphere.