  Colour-magnitude diagrams are presented for the first time for L32, L38, K28
(L43), K44 (L68) and L116, which are clusters projected onto the outer parts of
the Small Magellanic Cloud (SMC). The photometry was carried out in the
Washington system $C$ and $T_1$ filters allowing the determination of ages by
means of the magnitude difference between the red giant clump and the main
sequence turnoff, and metallicities from the red giant branch locus. The
clusters have ages in the range 2-6 Gyr, and metallicities between $-1.65<$
[Fe/H] $<-1.10$, increasing the sample of intermediate-age clusters in the SMC.
L116, the outermost cluster projected onto the SMC, is a foreground cluster,
and somewhat closer to us than the Large Magellanic Cloud. Our results,
combined with those for other clusters in the literature, show epochs of sudden
chemical enrichment in the age-metallicity plane, which favour a bursting star
formation history as opposede to a continuous one for the SMC.
