The typical scale and velocity of the dominant, turbulent eddies excited by the motion of galaxies in clusters are determined from basic considerations which are valid if a steady state is attained. Hydrodynamic turbulence in the intracluster plasma presumably generates magnetic fields; our estimates of the typical scale and mean strength of these fields in cluster cores are about 10 kpc and at most a few 10 −7 G. Implications of fields with these properties on the detectability of diffuse hard X-ray emission from clusters, and on transport properties in the intracluster space, are discussed