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We use Gaia DR3 data to study the Collinder 132-Gulliver 21 region via themachine learning algorithm StarGO, and find eight subgroups of stars (ASCC 32,Collinder 132 gp 1--6, Gulliver 21) located in close proximity. Three co-movingpopulations were identified among these eight subgroups: (i) a coeval 25Myr-old moving group (Collinder 132); (ii) an intermediate-age (50--100 Myr)group; and (iii) the 275 Myr-old dissolving cluster Gulliver 21. These threepopulations form parallel diagonal stripe-shape over-densities in the U--Vdistribution, which differ from open clusters and stellar groups in the solarneighborhood. We name this kinematic structure the Collinder 132-Gulliver 21stream, as it extends over 270 pc in the 3D space. The oldest populationGulliver21 is spatially surrounded by the Collinder 132 moving group and theintermediate-age group. Stars in the Collinder 132-Gulliver 21 stream have anage difference up to 250 Myr. Metallicity information shows a variation of 0.3dex between the youngest and oldest populations. The formation of theCollinder132-Gulliver 21 stream involves both star formation and dynamicalheating. The youngest population (Collinder 132 moving group) with homogeneousmetallicity is probably formed through filamentary star formation. Theintermediate-age and the oldest population were then scatted by the Galacticbar or spiral structure resonance to intercept Collinder 132's orbit. Withoutmutual interaction between each population, the three populations are flying byeach other currently and will become distinct three groups again inapproximately ~50Myr.

Dynamical Origin for the Collinder 132-Gulliver 21 Stream: A Mixture of three Co-Moving Populations with an Age Difference of 250 Myr