  Using high resolution Cluster satellite observations, we show that the
turbulent solar wind is populated by magnetic discontinuities at different
scales, going from proton down to electron scales. The structure of these
layers resembles the Harris equilibrium profile in plasmas. Using a
multi-dimensional intermittency technique, we show that these structures are
connected through the scales. Supported by numerical simulations of magnetic
reconnection, we show that observations are consistent with a scenario where
many current layers develop in turbulence, and where the outflow of these
reconnection events are characterized by complex sub-proton networks of
secondary islands, in a self-similar way. The present work establishes that the
picture of "reconnection in turbulence" and "turbulent reconnection",
separately invoked as ubiquitous, coexist in space plasmas.
