  In situ spacecraft data on the solar wind show events identified as magnetic
reconnection with outflows and apparent "`$X$-lines" $10^{3-4}$ times ion
scales. To understand the role of turbulence at these scales, we make a case
study of an inertial-range reconnection event in a magnetohydrodynamic (MHD)
simulation. We observe stochastic wandering of field-lines in space, breakdown
of standard magnetic flux-freezing due to Richardson dispersion, and a
broadened reconnection zone containing many current sheets. The coarse-grain
magnetic geometry is like large-scale reconnection in the solar wind, however,
with a hyperbolic flux-tube or "$X$-line" extending over integral
length-scales.
