We present a study of a recently discovered stellar overdensity near the northern edge of the Small Magellanic Cloud ( SMCNOD ) .
We exploited variable stars from the fourth release of the Optical Gravitational Lensing Experiment ( OGLE ) .
We used mainly pulsating variable stars and investigated their potential association with the SMCNOD using their spatial distribution and distances .
We found four rather spatially concentrated anomalous Cepheids and eight evenly dispersed RR Lyrae stars to be most likely members of this overdensity .
The anomalous Cepheids inside the SMCNOD trace possible intermediate-age population with ages ranging between 2 - 4.5 Gyr .
The age distribution of anomalous Cepheids seems to be in a good agreement with the age distribution of anomalous Cepheids in the SMC .
Using empirical relations for RR Lyrae stars we determined the median metallicity for a possible old population in the SMCNOD to be [ Fe / H ] _ { SMCNOD } = -1.71 \pm 0.21 dex , which is in agreement with median metallicity of the old SMC population .
The density profile for anomalous Cepheids shows a small anomaly at the position of the SMCNOD , on the other hand , RR Lyrae variables show no such deviation .
The probability of finding the observed number of variable stars at the location of the SMCNOD by chance is very low for anomalous Cepheids ( 0.7 % ) but high for RR Lyrae stars ( 13.0 % ) .
Based on its variable stars content , we thus confirm the presence of a modest overdensity in intermediate-age stars in the SMCNOD and conclude that it probably has its origin in the SMC rather than to be the remnant of an accreted dwarf galaxy .