The Sun's magnetic activity cycle of $\sim 22$ years involves a large-scale reversal of the polarity of the magnetic field every $\sim 11$ years.
There are very many observations of other solar-type stars that show, indirectly, they they too have magnetic activity cycles in the form of modulated emission of tracers of the magnetic field - starspots, chromospheric and coronal activity (e.g. Olah et al. 2016 and references therein).
To directly measure the reversing cycles in magnetic polarity requires spatially resolved maps of the vector magnetic field. Such spatially resolved maps are possible for fast-rotating, and hence highly magnetically active stars through Zeeman Doppler Imaging. In general, highly magnetically active stars appear not to show magnetic activity variations as strongly as the Sun. Nevertheless, recent instrumental developments have led to (difficult) observations of some solar-type stars with intermediate rotation rates. There is now plenty of evidence for magnetic polarity reversals in many of these (e.g. in Chi$^1$ Ori, Rosen et al. 2016; in LQ Hya, Lehtinen 2019; in V1358 Ori, Willamo et al. 2021).
Whilst the observations are not densely sampled enough to say for sure that this is cyclical behaviour following the same pattern as the Sun, the reversals have been found to correlate quite well with maxima or minima in the indirect indicators of magnetic activity.