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Filaments play an important role in star formation, but the formation processof filaments themselves is still unclear. The high-mass star forming clumpG286.21+0.17 (G286 for short) that contains an "L" type filament was thought toundergo global collapse. Our high resolution ALMA band 3 observations resolvethe gas kinematics of G286 and reveal two sub-clumps with very differentvelocities inside it. We find that the "blue profile" (an indicator of gasinfall) of HCO+ lines in single dish observations of G286 is actually caused bygas emission from the two sub-clumps rather than gas infall. We advise greatcaution in interpreting gas kinematics (e.g., infall) from line profiles towarddistant massive clumps in single dish observations. Energetic outflows areidentified in G286 but the outflows are not strong enough to drive expansion ofthe two sub-clumps. The two parts of the "L" type filament ("NW-SE" and "NE-SW"filaments) show prominent velocity gradients perpendicular to their major axes,indicating that they are likely formed due to large-scale compression flows. Weargue that the large-scale compression flows could be induced by the expansionof nearby giant HII regions. The "NW-SE" and "NE-SW" filaments seem to be incollision, and a large amount of gas has been accumulated in the junctionregion where the most massive core G286c1 forms.

ATOMS: ALMA Three-millimeter Observations of Massive Star-forming regions -- VI. On the formation of the "L" type filament in G286.21+0.17