  Weak Gravitational Lensing is a powerful probe of the dark sector of the
Universe. One of the main challenges for this technique is the treatment of
systematics in the measurement of cosmic shear from galaxy shapes. In an
earlier work, Refregier & Amara (2014) have proposed the Monte Carlo Control
Loops (MCCL) to overcome these effects using a forward modeling approach. We
focus here on one of the control loops in this method, the task of which is the
calibration of the shear measurement. For this purpose, we first consider the
requirements on the shear systematics for a given survey and propagate them to
different systematics terms. We use two one-point statistics to calibrate the
shear measurement and six further one-point statistics as diagnostics. We also
propagate the systematics levels that we estimate from the one-point functions
to the two-point functions for the different systematic error sources. This
allows us to assess the consistency between the systematics levels measured in
different ways. To test the method, we construct synthetic sky surveys with an
area of 1,700 deg$^2$. With some simplifying assumptions, we are able to meet
the requirements on the shear calibration for this survey configuration.
Furthermore, we account for the total residual shear systematics in terms of
the contributing sources. We discuss how this MCCL framework can be applied to
current and future weak lensing surveys.
