We develop a novel method of measuring the lensing distortion profiles of clusters
with stacking the ``scaled'' amplitudes of background galaxy ellipticities as a
function of the ``scaled¡Ç' centric radius according to the Navarro-Frenk-White (NFW)
prediction of each cluster, based on the assumption that the different clusters in a
sample follow the universal NFW profile.  We apply this method to the Subaru weak
lensing data and the {\it XMM}/{\it Chandra} X-ray observables for a sample of 50
massive clusters in the redshift range 0.15< z< 0.3$, where their halo masses range
over an order of magnitude.  To estimate the NFW parameters of each cluster, we use
the halo mass proxy relation of X-ray observables, based on either the hydrostatic
equilibrium or the gas mass, and then infer the halo concentration from the model
scaling relation of halo concentration  with halo mass.  We evaluate a performance of
the NFW scaling analysis by measuring the scatters of 50 cluster lensing profiles
relative to the NFW predictions over a range of radii, 0.14<R/[Mpc/h]< 2.8. We found a
4 - 6sigma level evidence of the universal NFW profile in 50 clusters, for both the
X-ray halo mass proxy relations, although the gas mass appears to be a better  proxy
of the underlying true mass. In this talk I will describe this new method and discuss
other applications to future data.