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The Tolman-Bondi-Lema\^itre type of inhomogeneous spacetime with generalisedChaplygin gas equation of state given by $p = -\frac{A}{\rho^{\alpha}}$ isinvestigated where $ \alpha$ is a constant. We get an inhomogeneous spacetimeat early stage but at the late stage of universe the inhomogeneity disappearwith suitable radial co-ordinate transformation. For the large scale factor ourmodel behaves like $\Lambda$CDM type which is in accord with the recent WMAPstudies. We have calculated $\frac{\partial \rho}{\partial r}$ and it is foundto be negative for $\alpha > 0$ which is in agreement with the observationalanalysis. A striking difference with Chaplygin gas ($ \alpha = 1$) lies in thefact that with any suitable co-ordinate transformation our metric cannot bereduced to the Einstein-de Sitter type of homogeneous spacetime as is possiblefor the Chaplygin gas. We have also studied the effective decelerationparameter and find that the desired feature of \emph{flip} occurs at the lateuniverse. It is seen that the flip time depends explicitly on $\alpha$. We alsofind that flip is not synchronous occurring earlier at the outer shells, thusoffering a natural path against occurrence of wellknown shell crossingsingularity. This is unlike the Tolman-Bondi case with perfect gas where onehas to impose stringent external conditions to avoid this type of singularity.We further observe that if we adopt separation of variables method to solve thefield equations the inhomogeneity in matter distribution disappears. The wholesituation is later discussed with the help of Raychaudhury equation and theresults compared with previous cases. This work is the generalisation of ourprevious article where we have taken $\alpha =1$.

Tolman-Bondi-Lema\^itre spacetime with a generalised Chaplygin gas