  We propose a scalar potential of inflation, motivated by modular invariant
supergravity, and compute the angular power spectra of the adiabatic density
perturbations that result from this model. The potential consists of three
scalar fields, S, Y and T, together with two free parameters. By fitting the
parameters to cosmological data at the fixed point T=1, we find that the
potential behaves like the single-field potential of S, which slowly rolls down
along the minimized trajectory in Y. We further show that the inflation
predictions corresponding to this potential provide a good fit to the recent
three-year WMAP data, e.g. the spectral index n_s = 0.951. The TT and TE
angular power spectra obtained from our model almost completely coincide with
the corresponding results obtained from the \LambdaCDM model. We conclude that
our model is considered to be an adequate theory of inflation that explains the
present data, although the theoretical basis of this model should be further
explicated.
