  Alongside magnetic reconnection, turbulence is another fundamental nonlinear
plasma phenomenon that plays a key role in energy transport and conversion in
space and astrophysical plasmas. From a numerical, theoretical, and
observational point of view there is a long history of exploring the interplay
between these two phenomena in space plasma environments; however, recent
high-resolution, multi-spacecraft observations have ushered in a new era of
understanding this complex topic. The interplay between reconnection and
turbulence is both complex and multifaceted, and can be viewed through a number
of different interrelated lenses - including turbulence acting to generate
current sheets that undergo magnetic reconnection (turbulence-driven
reconnection), magnetic reconnection driving turbulent dynamics in an
environment (reconnection-driven turbulence) or acting as an intermediate step
in the excitation of turbulence, and the random diffusive/dispersive nature of
magnetic field lines embedded in turbulent fluctuations enabling so-called
stochastic reconnection. In this paper, we review the current state of
knowledge on these different facets of the interplay between turbulence and
reconnection in the context of collisionless plasmas, such as those found in
many near-Earth astrophysical environments, from a theoretical, numerical, and
observational perspective. Particular focus is given to several key regions in
Earth's magnetosphere - Earth's magnetosheath, magnetotail, and
Kelvin-Helmholtz vortices on the magnetopause flanks - where NASA's
Magnetospheric Multiscale mission has been providing new insights on the topic.
