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We model the dynamical interaction between the Small and Large MagellanicClouds and their corresponding stellar cluster populations. Our goal is toexplore whether the lack of old clusters ($\gtrsim 7$ Gyr) in the SmallMagellanic Cloud (SMC) can be the result of the capture of clusters by theLarge Magellanic Cloud (LMC), as well as their ejection due to the tidalinteraction between the two galaxies. For this purpose we perform a suite ofnumerical simulations probing a wide range of parameters for the orbit of theSMC about the LMC. We find that, for orbital eccentricities $e \geq 0.4$,approximately 15 per cent of the SMC clusters are captured by the LMC. Inaddition, another 20 to 50 per cent of its clusters are ejected into theintergalactic medium. In general, the clusters lost by the SMC are the lesstightly bound cluster population. The final LMC cluster distribution shows aspatial segregation between clusters that originally belonged to the LMC andthose that were captured from the SMC. Clusters that originally belonged to theSMC are more likely to be found in the outskirts of the LMC. Within thisscenario it is possible to interpret the difference observed between the starfield and cluster SMC Age-Metallicity Relationships for ages $\gtrsim 7$ Gyr.

On a possible origin for the lack of old star clusters in the Small Magellanic Cloud