  Aim: We aim to estimate the age and reddening parameters of already
identified star clusters within the Small Magellanic Cloud (SMC) in a
consistent way using available photometric data, classify them based on their
mass and strength, and study their spatio- temporal distribution.
  Methods: We have used a semi-automated quantitative method, developed in the
first paper of this series (Paper I), to estimate the cluster parameters using
the V and I band photometric data from the Optical Gravitational Lensing
Experiment (OGLE) III survey.
  Results: We estimated parameters of 179 star clusters (17 newly
parameterised) and classified them into 4 groups. We present an online catalog
of parameters, and cleaned and isochrone-fitted Color Magnitude Diagrams of 179
clusters. We compiled age information of 468 clusters by combining previous
studies with our catalog, to study their spatio-temporal distribution. Most of
the clusters located in the southern part of the SMC are in the age range 600
Myr-1.25 Gyr, whereas, the clusters younger than 100 Myr are mostly found in
the northern SMC, with the central SMC showing continuous cluster formation.
The peak of the cluster age distribution is identified at 130 Myr, very similar
to the Large Magellanic Cloud (LMC) in Paper I.
  Conclusion: We suggest that the burst of cluster formation at 130 Myr is due
to the most recent LMC-SMC interaction. 90% of the studied sample is found to
have mass <1700 M_sun, suggesting that the SMC is dominated by low mass
clusters. There is a tentative evidence for compact clusters in the LMC when
compared to those in the Galaxy and the SMC. A progressive shifting of cluster
location from the South to North of the SMC is identified in last 600 Myr. The
details of spatio-temporal distribution of clusters presented in two videos in
this study can be used as a tool to constrain details of the recent LMC-SMC
interactions.
