  The Tolman-Bondi-Lema\^itre type of inhomogeneous spacetime with generalised
Chaplygin gas equation of state given by $p = -\frac{A}{\rho^{\alpha}}$ is
investigated where $ \alpha$ is a constant. We get an inhomogeneous spacetime
at early stage but at the late stage of universe the inhomogeneity disappear
with suitable radial co-ordinate transformation. For the large scale factor our
model behaves like $\Lambda$CDM type which is in accord with the recent WMAP
studies. We have calculated $\frac{\partial \rho}{\partial r}$ and it is found
to be negative for $\alpha > 0$ which is in agreement with the observational
analysis. A striking difference with Chaplygin gas ($ \alpha = 1$) lies in the
fact that with any suitable co-ordinate transformation our metric cannot be
reduced to the Einstein-de Sitter type of homogeneous spacetime as is possible
for the Chaplygin gas. We have also studied the effective deceleration
parameter and find that the desired feature of \emph{flip} occurs at the late
universe. It is seen that the flip time depends explicitly on $\alpha$. We also
find that flip is not synchronous occurring earlier at the outer shells, thus
offering a natural path against occurrence of wellknown shell crossing
singularity. This is unlike the Tolman-Bondi case with perfect gas where one
has to impose stringent external conditions to avoid this type of singularity.
We further observe that if we adopt separation of variables method to solve the
field equations the inhomogeneity in matter distribution disappears. The whole
situation is later discussed with the help of Raychaudhury equation and the
results compared with previous cases. This work is the generalisation of our
previous article where we have taken $\alpha =1$.
