Weak gravitational lensing is one of the most promising tools to investigate the equation-of-state of dark energy. In�order to obtain reliable parameter estimations for current and future experiments, a�good theoretical understanding of dark matter clustering is essential. Of�particular interest is the statistical precision to which weak lensing observables, such�as cosmic shear correlation functions, can be determined.

We construct a fitting formula for the non-Gaussian part of the covariance of the lensing power spectrum. The Gaussian contribution to the covariance, which is proportional to the lensing power spectrum squared, and optionally shape noise can be included easily by adding their contributions.

Starting from a canonical estimator for the dimensionless lensing power spectrum, we model first the covariance in the halo model approach including all four halo terms for one fiducial cosmology and then fit two polynomials to the expression found. On large scales, we use a first-order polynomial in the wave-numbers and dimensionless power spectra that goes asymptotically towards 1.1   for 0, i.e.,�the result for the non-Gaussian part of the covariance using tree-level perturbation theory. On the other hand, for small scales we employ a second-order polynomial in the dimensionless power spectra for the�fit.

We obtain a fitting formula for the non-Gaussian contribution of the convergence power spectrum covariance that is accurate to�10% for the off-diagonal elements, and to�5% for the diagonal elements, in the range 50 5000 nd can be used for single source redshifts z_s ∈ [0.5,2.0] in WMAP5-like�cosmologies.