A luminosity function for star clusters brighter than MB = -4.5 in the LMC is determined from eye estimates of the integrated magnitudes of all clusters in two large regions of the LMC. The differential luminosity function rises monotonically toward faint magnitudes. Except for a higher abundance of bright clusters, it is qualitatively similar to the luminosity function for the open clusters in the Galaxy. It does not have the single-peaked shape that characterizes the globular-cluster systems of the Galaxy and M 31. It is found that the total luminosity of the LMC cluster system is dominated by the brightest members while the fainter clusters contribute most to the total number.