The complexity and variability of plasma turbulence as observed in space is in part due to dynamics at many scales, ranging from macroscopic fluid scales to sub-electron scales. Depending on the plasma properties and the time and length scales of interest, a plasma can be described in various limits, such as kinetic and magnetohydrodynamic models. A common feature is the phenomenon of cross-scale energy transfer. This session discusses how plasma dynamics bridges multiple scales, what new ingredients are introduced as models progress from fluid to kinetic, and identification of key steps in energy transfer. Study of this transfer leads to better understanding of dissipation and heating, transport, field line wandering, and particle acceleration in the magnetosphere, solar wind and elsewhere in space. Contributions are welcome regarding energy spectra, cross-scale transfer, hierarchy of structures, intermittency, energy dissipation, refined similarity, and related processes, from theory, simulations, and/or observations from all relevant spacecraft.